Are All Non-Thermal Radio-Emitting O-Stars Binaries?

Details Are All Non-Thermal Radio-Emitting O-Stars Binaries? Are All Non-Thermal Radio-Emitting O-Stars Binaries?

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..361..515l&link_type=abstract

Active OB-Stars: Laboratories for Stellar and Circumstellar Physics, ASP Conference Series, Vol. 361, Proceedings of the confere

Physics

Scientific paper

We present qualitative models for the non-thermal radio emission of single O stars, in terms of synchrotron emission from relativistic electrons. These electrons are accelerated in shocks generated by the instability of the driving mechanism of the stellar wind. Hydrodynamical simulations show that wind-embedded shocks decay as they move outward with the flow. When we include this effect in our synchrotron models, we find that the observed non-thermal emission cannot be explained by synchrotron emission from wind-embedded shocks. The most likely alternative is that relativistic electrons are accelerated in shocks generated by the collision of two stellar winds. The non-thermal radio emitters are therefore all binary or multiple systems. This hypothesis is supported by periodic radio light curves of two presumably single O stars.

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